{"paper":{"title":"Constraining Wind-Driven Accretion Onto Gaia BH3 With Chandra","arxiv_id":"2406.07602","primary_cat":"astro-ph.HE","submitted_at":"2024-06-11T18:00:00+00:00","version_compiled":"v2"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v2","sentences":[{"i":0,"p":0.99,"id":"s0","own":false,"role":"background","text":"Gaia BH3 is the most massive known stellar-origin black hole in the Milky Way, with a mass $M_\\bullet \\approx 33 \\, \\rm M_\\odot$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.13,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.99,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.98,"id":"s1","own":false,"role":"background","text":"Detected from Gaia's astrometry, this black hole is in the mass range of those observed via gravitational waves, whose nature is still highly debated.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.1,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.18,"role_probabilities":{"gap":0.02,"method":0.0,"result":0.0,"background":0.98,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.96,"id":"s2","own":false,"role":"background","text":"Hosted in a binary system with a companion giant star that is too far away for Roche-lobe mass transfer, this black hole could nonetheless accrete at low levels due to wind-driven mass-loss from its companion star, thus accreting in advection-dominated accretion flow, or ADAF, mode.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.11,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.0,"background":0.96,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.01}},{"i":3,"p":0.95,"id":"s3","own":true,"role":"result","text":"Using stellar wind models, we constrain its Eddington ratio in the range $10^{-9} < f_{\\rm Edd} < 10^{-7}$, corresponding to radiative efficiencies $5\\times10^{-5} < \\epsilon < 10^{-3}$, compatible with radiatively inefficient accretion modes.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.88,"main_claim_p":0.24,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.95,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.03,"interpretation":0.01}},{"i":4,"p":0.98,"id":"s4","own":true,"role":"result","text":"Chandra ACIS-S observed this object and obtained the most sensitive upper bound of its [2-10] keV flux: $F_X < 3.25 \\times 10^{-15} \\, \\rm erg \\, s^{-1} \\, cm^{-2}$ at $90\\%$ confidence level corresponding to $L_{[2-10]}< 2.10 \\times 10^{29} \\, \\rm erg \\, s^{-1}$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.14,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":5,"p":0.98,"id":"s5","own":true,"role":"result","text":"Using ADAF emission models, we constrained its accretion rate to $f_{\\rm Edd}< 4.91 \\times 10^{-7}$ at the apastron, in agreement with our theoretical estimate.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.19,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.01}},{"i":6,"p":0.79,"id":"s6","own":true,"role":"result","text":"At the periastron, we expect fluxes $\\sim 50$ times larger.","hedge":{"p":0.47,"label":"hedged_possibility"},"own_p":0.71,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.79,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.2}},{"i":7,"p":0.98,"id":"s7","own":true,"role":"interpretation","text":"Because of the inferred low rates, accretion did not significantly contribute to black hole growth over the system's lifetime.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.76,"main_claim_p":0.4,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.98}},{"i":8,"p":0.82,"id":"s8","own":false,"role":"future_work","text":"Detecting the electromagnetic emission from Gaia BH3 will be fundamental to informing stellar wind and accretion disk 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